Prospects for Cosmic Axion Detection with ABRACADABRA

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1 Prospects for Cosmic Axion Detection with ABRACADABRA Jesse Thaler GPMFC Workshop on Ultralight Dark Matter, Washington, DC January 27, 2017 Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 1

A Broadband/Resonant Approach to Cosmic Axion Detection with an Amplifying B-field Ring Apparatus From Theory to Experiment ABRA 10cm r R a B 0 h [Kahn, Safdi, JDT, 1602.

2 A Broadband/Resonant Approach to Cosmic Axion Detection with an Amplifying B-field Ring Apparatus From Theory to Experiment ABRA 10cm r R a B 0 h [Kahn, Safdi, JDT, ] [development at MIT under NSF EAGER with PI Winslow, Conrad, Formaggio, Heine, Kahn, Minervini, Ouellet, Perez, Radovinsky, Safdi, JDT, Winklehner] Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 2

3 Ultimate Goal: ABRACADABRA 1m (or 10m) GUT-scale QCD Axion Dark Matter Strong CP solution at well-motivated mass scale f A (GeV) Dark Matter (pre-inflation PQ phase transition) XENON100 (g Aee, DFSZ) θ i = a i /f a Dark Matter (post-inflation PQ phase transition) Hot-DM / CMB / BBN ahtl initial misalignment 3H = m a a T 3/2 cos(m a t) NS in Cas A Hint (g Ann DFSZ) Telescope/EBL SN1987A (g App KSVZ) Burst Duration Beam Dump Counts in SuperK RG Hint RGs in GCs (g Aee DFSZ) and right DM abundance with 1% tuning in initial misalignment angle. t Black Holes HB Hint WDLF Hint WDLF (g Aee DFSZ) HB Stars in GCs (g Aγγ DFSZ) CASPEr ADMX ADMX G2 CAST IAXO Axion Mass m A (ev) [2016 PDG Axion Review] KSVZ T 250 khz Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 3

4 Initial Target: ABRACADABRA 10cm Axion-like DM coupled to Electromagnetism - CAST IAXO L g aγγ ae B = / Axion Coupling G Aγγ (GeV -1 ) SN 1987A LSW (OSQAR) Helioscopes (CAST) HESS Haloscopes (ADMX) KSVZ DFSZ Horizontal Branch Stars Axion Mass m A (ev) VMB (PVLAS) Telescopes ( - ) ABRA 10cm broadband ABRA 10cm resonant ( ) - - ( ) ADMX QCD Axion Band Substantial discovery potential for small scale prototype Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 4

5 Initial Target: ABRACADABRA 10cm ga (GeV -1 ) Axion-like DM coupled to Electromagnetism Solve Strong CP with Exponentially Large E&M Coupling? L 1 / g 10 aγγaf /2 1 µνf eµν CAST N-M=26 IAXO ABRA 10cm broadband N-M= KSVZ f a (GeV) ABRA 10cm resonant m a (ev) IAXO ADMX ABRA-Res ABRA-Broad CASPEr-II ADMX QCD Axion Band Axion Coupling G Aγγ (GeV -1 ) LSW (OSQAR) Helioscopes (CAST) A Clockwork Horizontal Branch Axion: Stars SN 1987A HESS ψ E,E c Haloscopes (ADMX) KSVZ DFSZ Axion Mass m A (ev) VMB (PVLAS) [Farina, Pappadopulo, Rompineve, Tesi, ] [based on Choi, Im, ; Kaplan, Rattazzi, ; Giudice, McCullough, ] [appears to evade misalignment bounds from Ariasa, Cadamuro, Goodsell, Jaeckel, Redondo, Ringwald, ] Substantial discovery potential for small scale prototype Telescopes ψ D,D c π 0 π 1 π M π N π N 1 Further motivation to cover full axion parameter space Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 5

6 ABRACADABRA: Cosmic Axion Detection Cold Axion DM Classical Field Oscillations 2ρDM m a 10 9 ev a(t)= m a sin(m a t) e.g. λ Comp 1km τ Comp few µs Local DM Velocity Spatial Coherence Temporal Coherence v DM ' 10 3 λ deb ' λ Comp v DM τ deb ' τ Comp v 2 DM (motivates Q~10 6 resonators) Key Experimental Feature: complementary to cavities like ADMX λ Comp R exp Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 6

7 Review of Axion Electrodynamics L g aγγ ae B Modified Maxwell Equations: r E = g aγγ ra B r E = B r B =0 t r B = g aγγ a t B+g aγγra E+ E t Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA [see, e.g., Sikivie, 1983; Wilczek, 1987] 7

8 Review of Axion Electrodynamics L g aγγ ae B Modified Maxwell Equations: r E = g aγγ ra B r E = B r B =0 t r B = g aγγ a Gradients suppressed by vdm ~ 10 3 E/ t suppressed for λcomp Rexp (MQS = magnetoquasistatic limit) t B+g aγγra E+ E t Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA [see, e.g., Sikivie, 1983; Wilczek, 1987] 8

9 Review of Axion Electrodynamics L g aγγ ae B Modified Maxwell Equations: r E = g aγγ ra B r E = B r B =0 r B response t r B = g aγγ a Gradients suppressed by vdm ~ 10 3 E/ t suppressed for λcomp Rexp (MQS = magnetoquasistatic limit) t B+g aγγra E+ E t Axion-Induced Effective Current: Parallel to external field Static External Field J eff = g aγγ p 2ρDM cos(m a t)b 0 Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA [see, e.g., Sikivie, 1983; Wilczek, 1987] 9

10 ABRACADABRA: Amplifying B-field Ring Apparatus I coil B response J eff B 0 0 [Kahn, Safdi, JDT, ] [for a related solenoidal design, see Thomas, Cabrera, 2010; Sikivie, Sullivan, Tanner, ] Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 10

11 ABRACADABRA: Amplifying B-field Ring Apparatus B response I coil J eff Detecting AC field where DC field is zero (essential for vibrational noise suppression) Small gap to avoid Meissner screening (superconducting coils) B 0 0 geometric factor, typically O(10%) Φ a (t)=g aγγ p 2ρDM cos(m a t) (B max V toroid G toroid ) [Kahn, Safdi, JDT, ] [for a related solenoidal design, see Thomas, Cabrera, 2010; Sikivie, Sullivan, Tanner, ] Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 11

12 ABRA 10cm: Prototype Toroid Design 3 cm 6 cm 12 cm Counter-wound NbTi superconducting coils (minimize fringe fields) Wire spacing sufficient for Meissner gap Not shown: shunt to allow injection of persistent current B 0 Bmax = 1 T Icoil = 120 A Vtoroid = 1020 cm 3 Gtoroid = Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 12

13 ABRA 10cm: Prototype Toroid Design 3 cm 6 cm Wire to inject test signal Support donut (perhaps 3D printed) Bmax = 1 T Icoil = 120 A Vtoroid = 1020 cm 3 Gtoroid = Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 13

readout circuit SQUID pickup + amplifier (shown:

14 ABRA 10cm: Prototype Toroid Design 3 cm 6 cm Superconducting pickup cylinder Minimize inductance with tall cylinder (advice from K. Irwin) Gap to force pickup current through SQUID To readout circuit SQUID pickup + amplifier (shown: Magnicon amplifier array) Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 14

Cryogenics & Shielding 25 cm Dilution Refrigerator: Oxford Instruments Triton 400 12 L

CUORE 0νββ R&D Magnetic Shielding: Ideally superconducting Multilayer NbTi/Nb/Cu sheet?

15 Cryogenics & Shielding 25 cm Dilution Refrigerator: Oxford Instruments Triton L working volume Cryogen-free Can run for weeks unattended 700 mk 50 mk 10 mk Day job: CUORE 0νββ R&D Magnetic Shielding: Ideally superconducting Multilayer NbTi/Nb/Cu sheet? Alternatively, In/Cu? Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 15

16 ABRACADABRA: A Broadband/Resonant Approach Minimize circuit noise for given axion mass Example from low-field MRI Broadband Dominated by SQUID noise Temperaturedependent crossover Resonant Dominated by thermal noise [figure adapted from Myers, et al., Journal of Magnetic Resonance, 2007; see related discussion in Jaeckel, Redondo, ] Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 16

17 Complementary Readout Strategies Lower Frequencies: Broadband Pickup Loop M L p L i L SQUID Superconducting circuit SQUID noise dominates S 1/2 Φ, Φ 0 / Hz Close to shot noise limit 1/f noise present at lower frequencies [also good for transients, see Axion DM 2016] Higher Frequencies: Resonant Δω M Pickup RLC circuit inevitable dissipation Pickup L Loop p L i C R L SQUID Q = ω 0 L circuit /R circuit Q-enhancement of signal but thermal noise dominates at 100 mk up to Q = 10 8 Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 17

18 Complementary Readout Strategies Lower Frequencies: Broadband g min aγγ lower mass longer coherence time ma t total 1/4 minimize inductance with tall geometry; optimal sensitivity scales like (Rexp) -5/2 Lcircuit 1 S 1/2 B max V toroid G Φ,0 toroid ρdm Higher Frequencies: Resonant g min aγγ depends on resonant scanning strategy 1 1/4 m a t e-fold s Lcircuit 1 B max V toroid G toroid ρdm want low T and high Q T Q Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 18

19 ABRACADABRA: Potential Future Reach = / = = = = = = = = = = = = IAXO ADMX 1 year sensitivity SNR 1 VB = Vtoroid Gtoroid ( - ) GUT-scale Broadband T < 60 mk 1/f 50 Hz Resonant T = 100 mk Q = 10 6 ( ) - - ( ) MQS approximation breaks down (precisely where ADMX begins) Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 19

20 ABRA 10 cm: Potential Reach in CAST = / 1 month sensitivity SNR 1 IAXO ( - ) Broadband Resonant QCD Axion Band ( ) ADMX Assumes SQUID or thermal noise dominates - - ( ) Not bad for a one liter frozen donut Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 20

The ABRACADABRA Collaboration @ MIT Janet Conrad, Joe Formaggio, Sarah Heine, Yoni Kahn (Princeton), Joe Minervini, Jonathan Ouellet, Kerstin Perez, Alexey Radovinsky, Ben Safdi, JDT, Daniel

21 The ABRACADABRA MIT Janet Conrad, Joe Formaggio, Sarah Heine, Yoni Kahn (Princeton), Joe Minervini, Jonathan Ouellet, Kerstin Perez, Alexey Radovinsky, Ben Safdi, JDT, Daniel Winklehner, Lindley Winslow (NSF EAGER PI) Anticipated timeline for ABRA 10cm: Magnet installation by May for Summer 2017 data taking Seeking broader collaboration for ABRA 1m! LNS Laboratory for Nuclear Science MIT Laboratory for Nuclear Science MIT Plasma Science & Fusion Center Superconducting Systems, Inc. Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 21

Key Challenges for ABRA 10cm: Noise, Noise, Noise SQUID Target: S 1/2 B ' 10 2 ft/ p Hz @ 250 khz Vibrational Noise?

22 Key Challenges for ABRA 10cm: Noise, Noise, Noise SQUID Target: S 1/2 B ' 10 2 ft/ p 250 khz Vibrational Noise? fringe field S 1/2 B ' (10 6 B max )S 1/2 displacement /R exp (see backup slide for environmental magnetic noise) already close to target Essential that pickup cylinder is in zero-field region Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 22

Future Challenges for ABRA 1m Cool a meter-sized experiment? Yes*: CUORE = 1.

@10 mk, but toroid @ 1 K? Achieve vibrational isolation?

Yes*: + = Cryogenic Current Comparators Dark Matter Radio [1411.7382, 1610.

23 Future Challenges for ABRA 1m Cool a meter-sized experiment? Yes*: CUORE = mk The Coldest Cubic Meter in the Known Universe But maybe mk, but 1 K? Achieve vibrational isolation? Yes*: Use LIGO-grade technology for 10 6 gain Optimize pickup geometry? Yes*: + = Cryogenic Current Comparators Dark Matter Radio [ , ] Pickup Snake Swallowing Its Tail Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 23

24 A Broadband/Resonant Approach to Cosmic Axion Detection with an Amplifying B-field Ring Apparatus Toroidal geometry with zero-field pickup Complementary readout strategies M Anticipated results from ABRA 10cm in 2017 L p L i L Δω M L p L i C R L Ultimate Goal: Probe GUT-scale QCD Axion Dark Matter Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 24

25 A Broadband/Resonant Approach to Cosmic Axion Detection with an Amplifying B-field Ring Apparatus Multiple Promising Strategies to Fully Explore QCD Axion f tion PQ 2.0 tion trapq 2.0 tion trapq 2.0 tion trapq 2.0tion trapost-inflation PQ 2.0 tion trapq trapq transition pre inflatio pre inflatio pre inflatio pre inflatio pre inflatio pre inflatio pre-inflation PQ transition na 1.5 na 1.5 na 1.5 na na na Hnatural valuesl 1.0 CASPEr Cold Cold Cold Cold Cold Cold Cold DM 1.0 BH super- CADABRA 0.0 radiance AD AD ADMX ADMX ADMX ADMX ADMX ADMX ADMX ABRA WD cooling hint ARIADNE ADMX-II Burst Duration Hg ae L Hot-DMêCMBêBBN Telescope ê EBL SK SN1987A Globular ClustersHg ag L White DwarfsHg ae L Hg ae L Solar Neutrino fluxhg ag L IAXO Helioscopes Beam Dump m [adapted from Essig et al., ] Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 25

26 Backup Slides Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 26

Key Challenges for ABRA 10cm: Noise, Noise, Noise SQUID Target: S 1/2 B ' 10 2 ft/ p Hz @ 250 khz Environmental Magnetic Noise?

27 Key Challenges for ABRA 10cm: Noise, Noise, Noise SQUID Target: S 1/2 B ' 10 2 ft/ p 250 khz Environmental Magnetic Noise? If you don t shield fully: With dedicated effort, target seems achievable x10 3 Jesse Thaler Prospects for Cosmic Axion Detection with ABRACADABRA 27

New experiment for axion dark matter

New experiment for axion dark matter J. Redondo and J. Jaeckel Feb 27th 2014 Outline - x-summary of Axion and ALP DM - Axion DM waves in Magnetic fields - Dish experiment - Understanding cavity experiments